The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Fulton, M.; Smartt, S. J.; Rhodes, L.; Huber, M. E.; Villar, A.; Moore, T.; Srivastav, Shubham; Schultz, A. S. B.; Chambers, K.; Izzo, L.; Hjorth, J.; Chen, Ting-Wan; Nicholl, M.; Foley, R. J.; Rest, A.; Smith, K.; Young, D. R.; Bright, J. S.; Zenati, Yossef; Boer, T. J. L. de; Bulger, J.; Fairlamb, J.; Gao, Hua; Lin, Chien-Cheng; Magnier, E. A.; Smith, I. A.; Wainscoat, R. J.; Coulter, D. A.; Jones, D. O.; Kilpatrick, C. D.; McGill, Peter; Ramírez-Ruiz, E.; Lee, Kyoung-Soo; Narayan, Gautham; Ramakrishnan, Vandana; Ridden-Harper, Ryan; Singh, Avinash; Wang, Q.; Kong, Albert; Ngeow, Chow-Choong; Pan, Y.-C.; Yang, S.; Davis, Kyle W.; Piro, Anthony L.; Rojas-Bravo, C.; J., Sommer,; Yadavalli, S. K.

doi:10.3847/2041-8213/acc101

Cited by 14 publications

(20 citation statements)

References 57 publications

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“…Due to the size of the parameter space, the log Bayes factor prefers the simpler top-hat jet model, 0.542 ± 0.140 for the Extended data and 0.540 ± 0.136 for the GRANDMA data (see Table 2). Hence, there is no strong evidence for or against the presence of an SN contribution consistent with the nugent-hyper model combined with the models used in our analysis (see, for instance, Fulton et al 2023 for another interpretation. jets have opening angles core  q (2°.5 ± 1°.0) (Wang et al 2018).…”

Section: Properties Of the Grb Afterglow From Bayesian Inferencementioning

confidence: 69%

“…The afterglow of GRB 221009A is clearly among the more luminous detected so far, but it is not egregious. Only at late times does the unbroken decay lead it to become exceptional, but we caution that these observations are not corrected for host-galaxy and SN contribution and are therefore to be taken with caution (see Fulton et al 2023 for the potential SN contribution, but see also Shrestha et al 2023).…”

Section: The Afterglow Of Grb 221009a In a Global Context: Luminous B...mentioning

confidence: 99%

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GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Канн

Agayeva

Aivazyan

et al. 2023

ApJL

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Object GRB 221009A is the brightest gamma-ray burst (GRB) detected in more than 50 yr of study. In this paper, we present observations in the X-ray and optical domains obtained by the GRANDMA Collaboration and the Insight Collaboration. We study the optical afterglow with empirical fitting using the GRANDMA+HXMT-LE data sets augmented with data from the literature up to 60 days. We then model numerically using a Bayesian approach, and we find that the GRB afterglow, extinguished by a large dust column, is most likely behind a combination of a large Milky Way dust column and moderate low-metallicity dust in the host galaxy. Using the GRANDMA+HXMT-LE+XRT data set, we find that the simplest model, where the observed afterglow is produced by synchrotron radiation at the forward external shock during the deceleration of a top-hat relativistic jet by a uniform medium, fits the multiwavelength observations only moderately well, with a tension between the observed temporal and spectral evolution. This tension is confirmed when using the augmented data set. We find that the consideration of a jet structure (Gaussian or power law), the inclusion of synchrotron self-Compton emission, or the presence of an underlying supernova do not improve the predictions. Placed in the global context of GRB optical afterglows, we find that the afterglow of GRB 221009A is luminous but not extraordinarily so, highlighting that some aspects of this GRB do not deviate from the global known sample despite its extreme energetics and the peculiar afterglow evolution.

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Section: Properties Of the Grb Afterglow From Bayesian Inferencementioning

confidence: 69%

Section: The Afterglow Of Grb 221009a In a Global Context: Luminous B...mentioning

confidence: 99%

GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Канн

Agayeva

Aivazyan

et al. 2023

ApJL

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“…As a result, in standard synchrotron afterglow theory, we do not expect the optical afterglow to decay with the same power-law index as the X-rays (e.g., Sari et al 1998). Thus, to remove the afterglow contribution we must model the optical decay separately from the X-rays (see Fulton et al 2023 and the first approach in Shrestha et al 2023).…”

Section: Previous Broadband Modeling Resultsmentioning

confidence: 99%

“…The unprecedented brightness led to extensive follow up across the electromagnetic spectrum (e.g., Fulton et al 2023;Laskar et al 2023;Kann et al 2023;O'Connor et al 2023;Williams et al 2023). Spectroscopy of the optical afterglow led to a redshift measurement of z = 0.151 (de Ugarte Postigo et al 2022a;Castro-Tirado et al 2022;Malesani et al 2023).…”

Section: Introductionmentioning

confidence: 99%

“…In Section 2 we report the observations of the optical afterglow of GRB 221009A; in Section 3 we analyze the observations, and statistically compare models with and without a SN component; in Section 4 we constrain the physical parameters of SN 2022xiw; in Section 5 we place GRB 221009A/SN 2022xiw in the context of the GRB-SN sample in the literature; and in Section 6 we summarize our conclusions. In the final stages of manuscript preparation, studies reporting conflicting results on the existence of SN emission were posted on the arXiv (Fulton et al 2023;Kann et al 2023;Levan et al 2023;Shrestha et al 2023)-where relevant we highlight differences in our approach and contrasts in our results.…”

Section: Introductionmentioning

confidence: 99%

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A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

Srinivasaragavan

O’Connor

Cenko

et al. 2023

ApJL

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We report observations of the optical counterpart of the long gamma-ray burst GRB 221009A. Due to the extreme rarity of being both nearby (z = 0.151) and highly energetic (E γ,iso ≥ 1054 erg), GRB 221009A offers a unique opportunity to probe the connection between massive star core collapse and relativistic jet formation across a very broad range of γ-ray properties. Adopting a phenomenological power-law model for the afterglow and host galaxy estimates from high-resolution Hubble Space Telescope imaging, we use Bayesian model comparison techniques to determine the likelihood of an associated supernova (SN) contributing excess flux to the optical light curve. Though not conclusive, we find moderate evidence (K Bayes = 101.2) for the presence of an additional component arising from an associated SN, SN 2022xiw, and find that it must be substantially fainter (<67% as bright at the 99% confidence interval) than SN 1998bw. Given the large and uncertain line-of-sight extinction, we attempt to constrain the SN parameters (M Ni, M ej, and E KE) under several different assumptions with respect to the host galaxy’s extinction. We find properties that are broadly consistent with previous GRB-associated SNe: M Ni = 0.05–0.25 M ⊙, M ej = 3.5–11.1 M ⊙, and E KE = (1.6–5.2) × 1052 erg. We note that these properties are weakly constrained due to the faintness of the SN with respect to the afterglow and host emission, but we do find a robust upper limit on M Ni of M Ni < 0.36 M ⊙. Given the tremendous range in isotropic gamma-ray energy release exhibited by GRBs (seven orders of magnitude), the SN emission appears to be decoupled from the central engine in these systems.

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JWST detection of a supernova associated with GRB 221009A without an r-process signature

Blanchard,

Villar,

Chornock

et al. 2024

Nat Astron

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Identifying the sites of r-process nucleosynthesis, a primary mechanism of heavy element production, is a key goal of astrophysics. The discovery of the brightest gamma-ray burst (GRB) to date, GRB 221009A, presented an opportunity to spectroscopically test the idea that r-process elements are produced following the collapse of rapidly rotating massive stars. Here we present James Webb Space Telescope observations of GRB 221009A obtained +168 and +170 rest-frame days after the gamma-ray trigger, and demonstrate that they are well described by a SN 1998bw-like supernova (SN) and power-law afterglow, with no evidence for a component from r-process emission. The SN, with a nickel mass of approximately 0.09 M⊙, is only slightly fainter than the brightness of SN 1998bw at this phase, which indicates that the SN is not an unusual GRB-SN. This demonstrates that the GRB and SN mechanisms are decoupled and that highly energetic GRBs are not likely to produce significant quantities of r-process material, which leaves open the question of whether explosions of massive stars are key sources of r-process elements. Moreover, the host galaxy of GRB 221009A has a very low metallicity of approximately 0.12 Z⊙ and strong H2 emission at the explosion site, which is consistent with recent star formation, hinting that environmental factors are responsible for its extreme energetics.

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The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Cited by 14 publications

References 57 publications

GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

A Sensitive Search for Supernova Emission Associated with the Extremely Energetic and Nearby GRB 221009A

JWST detection of a supernova associated with GRB 221009A without an r-process signature

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